The Incoherent Dynamo in Realistic Accretion Disks

Details The Incoherent Dynamo in Realistic Accretion Disks The Incoherent Dynamo in Realistic Accretion Disks

Dec 1997

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997aas...19111016v&link_type=abstract

American Astronomical Society, 191st AAS Meeting, #110.16; Bulletin of the American Astronomical Society, Vol. 29, p.1389

Astronomy and Astrophysics

Astronomy

Scientific paper

Recent work on cooling waves in accretion disks has shown that the mechanism for generating angular momentum transport scales with the local geometry of the disk as ~ (H/r)(n) , where n is approximately 3/2. If angular momentum transport is caused by local instabilities of the magnetic field, this implies a dynamo process which is both local and dependent on geometry. The incoherent alpha -Omega dynamo satisfies this criterion, since it arises from random fluctuations in the large scale helicity, creates axisymmetric magnetic domains, and is sensitive to the value of H/r through the height to circumference ratio of such domains. Here we explore the prospects for generating a quantitative agreement between the light curves of SXTs and dwarf novae and the predictions of this theory. We also discuss the constraints imposed by the current generation of numerical experiments.

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